When we decrease the \(\rho _s\)  (and consequently \(u\) ) the
deflection angle increases. At some points, the deflection angle
exceeds from \(2\pi \)  so that the light ray will make a complete loop
around the compact object before reaching at the observer. By
decreasing \(\rho _s\)  further, the photon will wind several times
around the black hole before emerging. Finally, for
\(\rho _s=\rho _{sp}\)  the deflection angle diverges and the photon is
captured by the black hole. Moreover, from equations (REF )
and (REF ), we can find that in the Charged Squashed
Kaluza-Klein Gödel black hole, both of the deflection angles
depend on the parameters \(j\) , \(\rho _0\)  and \(\rho _q\) , which implies
that we could detect the rotation of universe, the extra dimension
and charge of black hole in theory by gravitational lens. Note that
the \(I_\phi (\rho _s)\)  depend on \(j^2\) , not \(j\) . It
shows that the deflection angle is independent of the direction of rotation of universe.
But, from equation (REF ) we find that the integral
\(I_\psi (\rho )\)  contains the factor \(j\) , then the deflection angle
\(\alpha _\psi (\rho _s)\)  for the photon traveling around the lens
in two opposite directions is different .The main
reason is that the equatorial plan is parallel with Gödel
rotation plan [1]}. When \(j\)  vanishes, the deflection
angle of \(\psi \)  tends zero [2]}, [3]}. We focus on the deflection angle in the \(\phi \)  direction,
